Chelyabinsk superbolide explosion in the Earth’s atmosphere: A common phenomenon or unique coincidence?

The paper analyzes the disintegration of small cosmic bodies in a planetary atmosphere and most important facts observed during the fall of the Chelyabinsk superbolide: its speed loss during passage through the upper atmosphere, its strength and the character of destruction, the altitude of its explosion, and the energy release. Detailed data are presented on the aerodynamic phenomena accompanying the supersonic atmospheric entry and destruction of the superbolide. The strength of the original meteorite is evaluated as a function of its initial disintegration altitude. Principal data obtained on the collision between comet Shoemaker-Levy 9 and Jupiter are reported.     

Raman identification of calcite grains in the Chelyabinsk meteorite

Samples of the Chelyabinsk meteorite fallen in February 15, 2013, near Chelyabinsk, Russia, are analyzed by Raman spectroscopy. Olivines (forsterite), orthopyoxenes (enstatite), plagioclases (albite), iron oxides and sulfides, as well as calcite and, possibly, parisite were identified among mineral phases. Results were verified using scanning electron microscope with an energy-dispersive system (SEM-EDX). Data were compared with available materials on calcites from ordinary meteorites.     

Fragments of the Chelyabinsk meteorite shower: Distribution of masses and sizes and constraints on the mass of the largest fragment

This paper reports data on the masses of fragments of the Chelyabinsk meteorite shower (fall of 15.02.2013). Assuming a lognormal distribution for the masses of fragments, the logarithm of the mean mass and standard deviation were estimated for the available data, describing the distribution density of masses and calculated diameters of fragments. Based on the dependence of the cumulative number of fragments with masses equal or greater than a given value, the mass of the largest fragment of the Chelyabinsk meteorite shower was estimated. It was shown that the most probable mass of such a fragment is hundreds of kilograms for a total mass of infalling material of 100 metric tons (t) and 1–2 t for a total mass of 1000 t, and the lower constraint for the maximum mass of the fragment is a few tens of kilograms.     

Analytical results for the material of the Chelyabinsk meteorite

This paper presents the results of the mineralogical, petrographic, elemental, and isotopic analysis of the Chelyabinsk meteorite and their geochemical interpretation. It was shown that the meteorite can be assigned to LL5-group ordinary chondrites and underwent moderate shock metamorphism (stage S4). The Chelyabinsk meteorite contains a significant fraction (approximately one-third by volume) of shock-melted material similar in composition to the main volume of the meteorite. The results of isotopic analysis suggest that the history of meteorite formation included an impact event approximately 290 Ma ago.     

碰撞作用与类地行星起源探讨

类地行星挥发性元素普遍亏损很可能是由于太阳星云早期剧烈的太阳活动引起的。当气体、尘粒、挥发性元素和水被驱赶出内太阳系时，只有米级到公里级的物质保存下来并堆积成星子，最终吸积星子形成类地行星。我们认为类地行星的初始物质主要是已分异的星子和一些未分异的球粒陨石质星子或不同类型的陨石母体，最靠近太阳形成的星子具有最低的ＦｅＯ／（ＦｅＯ＋ＭｇＯ）值，水星是在靠近太阳的高度还原条件下吸积成分类似ＥＨ球粒陨石的星子形成的。地球的初始物质为分异的铁陨石及Ｈ群球粒陨石。随着距太阳距离增大及温度降低，陨石形成的部位大致为：ＥＨ、ＥＬ－ＩＡＢ－ＳＮＣ（辉玻无球粒陨石、辉橄无球粒陨石、纯橄无球粒陨石）－Ｅｕｃ（钙长辉长无球粒陨石）－Ｈ、Ｌ、ＬＬ－ＣＶ、ＣＭ、ＣＯ－Ｃｌ－彗星。物体之间、星子之间及行星与星子之间的碰撞对太阳系的形成和演化起着重要的作用。     

First find of srilankite in the Urals

The first find of srilankite (very rare Zr and Ti oxide, Ti₂ZrO₆) in the Urals and the third find in Russia is reported. Srilankite forms very small (0.5–20 μm) inclusions in some rutile grains. These minerals are observed in the rare rock variety, corundum-bearing spinel–saphirine hornblendite forming a block in serpentinized amphibolizied peridotite of the Ilmeny–Vishnevogorsk Complex, near the village of Taiginka, Chelyabinsk oblast. Srilankite has not been observed in such an association yet. The composition of the host rock provides evidence for its deep (the lowermost crust of the Earth) origin. Srilankites of the Urals are distinguished from all others by the high concentrations of UO₂, ThO₂, HfO₂, and Nb₂O₅, which provides additional evidence for their crustal origin. Srilankite may indicate high-temperature and high-pressure conditions of rock formation.     

Enstatite achondrite meteorites (aubrites) and the histories of their asteroidal parent bodies

The aubrites are nearly monomineralic enstatite pyroxenites, consisting mostly of nearly FeO-free enstatite, with minor albitic plagioclase, nearly FeO-free diopside and forsterite, metallic Fe,Ni, troilite, and a host of rare accessory minerals, many unknown from Earth, that formed under highly reducing conditions. As a result, many of the normally lithophile elements such as Ti, Cr, Mn, Na, etc. behave partly as chalcophiles (i.e., occur in sulfides), and Si is partly siderophile and occurs in metallic Fe,Ni. Aubrites must therefore have formed in a very unique part of the solar nebula, possibly within 1 AU of the Sun. While of the 27 aubrites, 15 are fragmental breccias, 6 are regolith breccias, and 6 are described as non-brecciated, their ingredients are clearly of igneous origin and formed by melting and fractional crystallization, possibly of a magma ocean. This is indicated by the occurrence of a variety of lithic clasts of igneous origin, and by the REE and other trace element distributions. Their highly reduced nature and their oxygen isotopic compositions suggest close kinship to the enstatite chondrites. However, they did not form from known EH or EL chondrites on their parent bodies. Rather, they formed from enstatite chondrite-like material on at least two separate parent bodies, the Shallowater parent body and, for all other aubrites, on the aubrite parent body. Visible and near-infrared reflectance spetra of asteroids suggest that the aubrite parent bodies may be asteroids of the E-type and perhaps the E(II) sub-class, such as 3103 Eger and 2867 Steins (the target of the Rosetta Mission). If aubrites formed by the melting and fractional crystallization of enstatite chondrite-like parent lithologies, which should have contained ～10 vol% plagioclase, then meteorites of enstatite-plagioclase basaltic composition should exist, which is not the case. These early basaltic melts may have been removed from the aubrite parent body by explosive pyroclastic volcanism, and these small pyroclasts would have been destroyed in space long ago. Age dates suggest that the aubrites formed very early in the history of the solar system, within a few Ma of CAI formation, and that the heat sources for heating and melting of their parent bodies were, most likely, short-lived radionuclides such as ²⁶Al and, perhaps, ⁶⁰Fe. Finally, attention has been drawn to the surface composition of Mercury of low bulk FeO and of nearly FeO-free enstatite, perhaps with plagioclase, diopside and sulfide. While known aubrites clearly did not originate from Mercury, recent calculations suggest that several percent of high-speed ejecta from Mercury reach Earth. This is only factors of 2–3 less than typical launches from Mars and, since there are now 53 Martian meteorites in our collections, meteoriticists should be alert to the potential discovery of a genuine meteorite from Mercury which, superficially, should resemble aubrites. However, recent results from the Neutron Spectrometer of the Messenger Flyby of Mercury have been interpreted to suggest that the planet’s surface may, in fact, contain abundant Fe–Ti-oxides and, if true, a meteorite from Mercury should not resemble any currently known meteorite type.     

东天山康古尔金矿床成矿物源的同位素地球化学特征

康古尔金矿床属晚古生代火山岩区剪切带蚀变岩型金矿。同位素地球化学研究表明,矿石中铅为正常铅,热液系统硫同位素组成为陨石硫型,矿石中碳、钕同位素组成具深源特征,同时矿石与火山岩围岩中的Ｓｉ、Ｓｒ、Ｓ、Ｐｂ等同位素组成相近,说明成矿物质主要来自矿体围岩———火山岩,晚期有少量来自矿区附近的侵入岩。铅、锶同位素组成反映成矿过程中也有少量壳源物质的加入。     

论全球岩石圈板块构造的动力学机制

全球板块构造的动力学机制问题是一个热门但至今尚未解决的难题。本文首先回顾了近百年来大地构造学的各种主要假说和近四十年来板块构造学说的许多新进展。在上述研究的基础上, 受Rampino和Stothers关于陨击作用可引起地表重大灾变事件思想的启发,笔者提出了一个新的假说。基于中、新生代(200 Ma以来)每隔33 Ma太阳系就会穿越一次银河系星际物质密集的银道面,诱发太阳系内部引力场的巨变,使部分小行星失稳,从而撞击地球。笔者根据用以描述中生代以来全球板块构造的七种不同的运动模式, 提出了巨大陨星在不同地点、以不同角度撞击地表岩石圈,可能诱发地幔底辟的形成,从而推动板块呈放射状或单向运移的假说,也即在200、170、100、65和0.78 Ma等时期的陨击事件基本上是垂直地表面而撞击的,从而诱发地幔底辟的形成和岩石圈板块的放射状张裂和运移;138 Ma的陨击事件可能是指向印度板块的斜向撞击;而35 Ma时期的微玻璃陨石撞击事件则是陨石以极低角度撞击地球表面的表现。陨石撞击地球,这是太阳系内部各星体之间引力作用变化的表现,因而此假说不是什么外因作用论。     

Analysis of selected samples of the Chelyabinsk meteorite for organic compounds by synchronous spectrofluorimetry

Analyses of some samples of the Chelyabinsk meteorite suggest that the meteoritic material can contain a mixture of complex organic compounds.     

The P-Wave Focusing Effect in a Low-Velocity Core of the Earth: Analytical Solution

This paper reports the calculation data on wave fields for the Earth’s model including the mantle and external and internal core with real parameters. The investigation has made it possible to identify physical phenomenon unknown previously such as the formation of the wave field focusing region in the Earth, emerging to the day surface before the first PKP-wave. This is due to the fact that spherical bodies (in this case, the low-velocity core of the Earth) are characterized by the collecting lens properties.

     

Ground penetrating radar investigation of the supposed fall site of a fragment of the Chelabinsk meteorite in Lake Chebarkul’

The bottom of Lake Chebarkul’ was investigated by ground penetrating radar at the fall site of a large fragment of the Chelyabinsk meteorite. Linear profiles and 3D reconstructions revealed an anomalous depression of the lake floor relief and the disturbance of the structure of the ice cover, which indicate the possible place of meteorite fragment occurrence.     

The substance of the Chelyabinsk meteorite: Results of geochemical and thermomagnetic studies

The fragments of the Chelyabinsk meteorite studied are represented by light-gray granular rock of chondritic structure. The chondrules and their cementing matter are mainly constituted by olivine and orthopyroxene. The matrix consists of a pyroxene-olivine aggregate with plagioclase, apatite, melted glass, and the inclusions of ore minerals: taenite, kamacite, troilite, pyrrhotite and pentlandite (more rarely), and individual grains of chromite and ilmenite. The comparison of the composition of the Chelyabinsk meteorite to the average composition of LL chondrites had shown their complete convergence. The concentrations of sidero- and chalcophile rare elements in the meteorite, normalized to CI chondrites, are much close to the values for LL chondrites and almost reproduce the character of their distribution in the spider diagram. However, some high-charged and lithophile elements (Nb, Zr, Hf, Sr, Ba, Th, and U) not belonging to the mentioned groups are characterized by somewhat increased contents. The enrichment of the samples of the Chelyabinsk meteorite in rare-earth elements compared to LL chondrite (5.18 against 3.58 ppm) is also revealed. This is related to the higher concentrations of light lanthanides in the meteorite samples, which is seen from the increased La/Yb ratio compared to the value for LL chondrite (1.9–2.3 and 1.4, respectively). Iron-nickel alloys are the main magnetism carriers in the Chelyabinsk meteorite. The compositions of kamacite, taenite, chromite, and Fe-sulfides are not much different. The optical and microprobe data are confirmed by the thermomagnetic parameters as well: (1) The specific magnetization of 4–6 Am²/kg points to small variations in the concentrations of magnetic minerals. (2) The M(T) curves for all the samples nearly repeat each other, and the Curie temperatures of 490–520 and 740–770°C are registered in the curves of the first and second heating, hence, these curves correspond to kamacite of various composition, right up to pure iron. (3) The monocline ferrimagnetic pyrrhotite of T_C = 320–340°C is registered in the treated fragments in both the M(T) curves of heating and cooling. (4) The concentrations by thermomagnetic analysis amount to 0.6–1.6% (0.9% average) for kamacite, 0.7–1.5% (1.1% average) for taenite, and 0–1.5% (0.4% average) for monocline pyrrhotite. (5) No magnetite was found in the M(T) curve during the first heating of the samples. Hence, the content of magnetite is much below 0.1.     

The Chelyabinsk meteoroid: A seismologist’s view

This work determines the parameters of the meteoroid that exploded in Chelyabinsk oblast on February 15, 2013. Using video observation and automobile registration cameras, we identified the trajectory and velocity of the meteoric body from the beginning of its glow to the destruction. The precise explosion time (03:20:34UTC) was determined on the basis of records of the broadband seismic stations and arrivals of the surface wave. The estimated explosion energy with assumption of a point source similar to a high thermonuclear explosion was 100 kt in TNT equivalent based on the surface wave amplitude. The archive of records of seismic stations during the meteorite flight is composed.     

类地天体与地球地质作用的比较研究

<正> 一、概述 地球是作为一员星球在银河系中运动和发展的。因而,它的形成和演化是应服从于一般星球形成和演化规律的。特别是与地球相邻近,而且特征也相近的星球,在形成和演化方面应有更多共同特点。 比较法是认识、鉴别事物的重要方法。事物是从与其他事物比较中反映出它的特性和共性的,在现在科学水平上,能与地球相比较的天体在亿万星球中还是极少数,我们将这些与地球相邻近,而特征又近似的天体称类地天体。     

车里雅宾斯克(Chelyabinsk)陨石的岩石矿物特征与冲击变质作用

2013年2月15日,俄罗斯车里雅宾斯克(Chelyabinsk)发生了伴随罕见的空中爆炸的大规模陨石雨事件。本文对3块代表不同冲击变质程度的车里雅宾斯克陨石碎块进行了研究。它们都具有部分熔壳,其中1块仅出现碎裂,1块含有冲击熔融细脉,1块基本由冲击熔融囊和冲击熔脉组成。冲击变质程度最低的样品,代表了该陨石母体小行星的原始岩石矿物学特征:即具有粗粒的岩石结构和均一的矿物化学组成,但仍保留一些残余球粒,表明受到了明显的热变质作用,其岩石类型可划分为5型。铁镁质硅酸盐高的Fe O含量(橄榄石Fa:27.9mol%~28.2mol%,辉石Fs值:23.3mol%~23.7mol%)、以及较低的Fe-Ni金属含量,表明其化学群属于低铁低金属的LL群。我们所分析的样品与前人报导的结果相似,未发现不同岩性的岩屑,表明车里雅宾斯克陨石的原始岩矿特征较为均一。3块陨石碎块中,随着冲击程度的增强,其冲击变质特征依次表现为硅酸盐矿物的破碎、熔长石化更为普遍、陨硫铁与铁镍合金共熔、硅酸盐熔脉的形成、铬铁矿与长石共熔、以及大量熔融囊的发育等。但是,在冲击熔融囊和熔脉中,以及相邻围岩中均未发现高压矿物相。熔脉中的橄榄石晶屑和相邻围岩的橄榄石颗粒表现为化学成分的不均一,在背散射电子图像中呈不同灰度的结构。这与其他强烈冲击变质陨石中橄榄石的林伍德石或瓦茨利石相变相似。该陨石中林伍德石或瓦茨利石的缺失很可能是由于强烈撞击后高温产生的退变质。这也表明车里雅宾斯克陨石的母体小行星可能遭受了非常强烈的撞击事件。     

The convincing identification of terrestrial meteorite impact structures: What works,what doesn't,and why

In the geological sciences it has only recently been recognized how important the process of impact cratering is on a planetary scale, where it is commonly the most important surface-modifying process. On the Moon and other planetary bodies that lack an appreciable atmosphere, meteorite impact craters are well preserved, and they can commonly be recognized from morphological characteristics, but on Earth complications arise as a consequence of the weathering, obliteration, deformation, or burial of impact craters and the projectiles that formed them. These problems made it necessary to develop diagnostic criteria for the identification and confirmation of impact structures on Earth. Diagnostic evidence for impact events is often present in the target rocks that were affected by the impact. The conditions of impact produce an unusual group of melted, shocked, and brecciated rocks, some of which fill the resulting crater, and others which are transported, in some cases to considerable distances from the source crater. Only the presence of diagnostic shock-metamorphic effects and, in some cases, the discovery of meteorites, or traces thereof, is generally accepted as unambiguous evidence for an impact origin. Shock deformation can be expressed in macroscopic form (shatter cones) or in microscopic forms (e.g., distinctive planar deformation features [PDFs] in quartz). In nature, shock-metamorphic effects are uniquely characteristic of shock levels associated with hypervelocity impact. The same two criteria (shock-metamorphic effects or traces of the impacting meteorite) apply to distal impact ejecta layers, and their presence confirms that materials found in such layers originated in an impact event at a possibly still unknown location. As of 2009 about 175 impact structures have been identified on Earth based on these criteria. A wide variety of shock-metamorphic effects has been identified, with the best diagnostic indicators for shock metamorphism being features that can be studied easily by using the polarizing microscope. These include specific planar microdeformation features (planar fractures [PFs], PDFs), isotropization (e.g., formation of diaplectic glasses), and phase changes (high pressure phases; melting). The present review provides a detailed discussion of shock effects and geochemical tracers that can be used for the unambiguous identification of impact structures, as well as an overview of doubtful criteria or ambiguous lines of evidence that have erroneously been applied in the past.     

火星生命研究的进展与前景

关于火星是否存在或曾经存在生命的争论由来已久。有人以ALH84001火星陨石新鲜破裂面上的大量碳酸盐小球体和多环芳香烃（PAHs）为主要依据，推论火星至少在13～36亿 aBP前很可能有生命形态存在。然而，很多人认为ALH84001陨石的各种特性可以是非生物成因的。由于地球上的生物在超过115℃的温度下很难存活（火星可与之类比），争论的焦点逐渐集中在碳酸盐球体的形成温度上。也有研究者关注该陨石上有机物质的来源问题。对ALH84001陨石的综合学科研究提出了互相矛盾的证据。综述了自1996年以来在国外各种主要期刊上发表的关于 ALH84001陨石与火星生命的研究成果（也包括了一些对其他火星陨石的研究），认为目前尚不能断言火星生命存在与否。对火星继续深入探索以获取进一步的证据是十分必要的。以美国国家航空和宇航局（NASA）Odys sey宇宙飞船起始的火星探测计划将引发新一轮火星生命研究的热潮。     

陨石氧同位素组成及其地学意义

介绍了各类陨石氧同位素组成的特点,对陨石氧同位素组成的主要成因观点进行了评述,结合地球的原始物质组成,讨论了陨石氧同位素组成的地球科学意义。